In this section, we analyse the effect of the AGN contribution on four of the most commonly
used morphological diagnostic diagrams, that we selected since they
have been broadly used in previous studies to separate between
different morphological types [1]}, [2]}, [3]}, [4]}, [5]}, [6]}, [7]}, [8]}, [9]}, [10]}, [11]}, [12]}, [13]}, [14]}, [15]}. Figures REF  to
REF  show the following diagrams: ASYM vs. CABR, CABR
vs. GINI, CCON vs. CABR, and CCON vs. M20, respectively. In each
figure, we represent the original local sample of non-active galaxies (top-left plot), and simulated
active galaxies with added 5% (top-right), 10% (middle-left), 25%
(middle-right), 50% (bottom-left), and 75% (bottom-right) of AGN
contribution to the total flux. In all plots we represent the location
of early-type (red), early-spiral (blue), late-spiral (green), and peculiar (magenta) galaxies.
The distribution of each parameter for the four morphological types are also represented as attached histograms on the top and to the right axes of each diagram.
In line with the results obtained in the previous two
sections, in general, it can be observed that for up to 10% of AGN contribution the
distribution of simulated galaxies does not change significantly in
comparison to the original samples. However, starting from 25% of AGN
contribution larger contamination can be observed between different
morphological types. Mix between early- and late-types becomes
significantly larger when having strong AGN contribution of 50% and
75% to the total galaxy flux, making difficult the separation between these two types as discussed more in Sec. . For easier comparison with the original sample, in all histograms, as a reference we introduced the vertical lines that correspond to the median values of parameters of different morphological types. Quantification for each parameter is given in Table REF .
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